Some regularities in the relationship of limb coronal mass ejections with eruptive prominences and post-eruptive arcades

A positive correlation is shown to exist between the angular sizes (in the sky plane) of eruptive prominences and/or post-eruptive arcades and coronal mass ejections (CMEs) associated with them. New regularities are found that characterize the relationship between the latitude of eruptive prominences (post-eruptive arcades) and the latitude position of CMEs associated with them in the field of view of a coronagraph. An interpretation of these regularities is given.     

Coronal mass ejections in July 2005 and an unusual heliospheric event

Using the events in July 2005 as an example, the causes and peculiarities of Forbush effects produced by solar sources remote from the central zone are discussed. The event in question differs from other effects observed at the periphery of interplanetary disturbances by strong variations in cosmic rays on the background of weak disturbances in the solar wind and magnetic field of the Earth. The cloud of magnetized plasma ejected from the Sun was large and fast, but it passed to the west from the Sun-Earth line. According to performed estimates, the mass of the ejected substance was close to the upper boundary of mass for coronal mass ejections (CMEs). Anomalous parameters and high modulation capability of the formed solar wind disturbance are explained, in particular, by the fact that it combined several CMEs and that the last fast disturbance was prepared by a series of impulsive events in the active region of the Sun. Usually, such a great mass is ejected directly after the main energy release in strong solar flares. In the given case, a powerful MHD disturbance occurred approximately half an hour after a maximum of hard X-ray burst under the conditions when gas pressure in the flare loops became close to magnetic pressure, which was just a premise of the largescale ejection.     

Topological model of the solar event including a flare and coronal mass ejection on October 19, 2001

Based on the analysis of a strong solar flare X1.6/2B on October 19, 2001 in the active region 9661, accompanied by a coronal mass ejection (CME) of the halo type, a topological model of development of this solar event is suggested. The model considers a unified process of development of CME and a chromosphere flare. According to the model, this process has a common source of energy supply: the turbulent current layer lying between the arcade of flare loops and the surface of CME going away. The structures on the ends of flare bands (SEFB) represent in this model chromosphere feet of the system of large-scale coronal magnetic arches at the initial stage of the dynamic processes whose evolution results in CME. Peripheral structures (PS) of the flare (elongated double bright emission strips beyond the limits of the active region) are interpreted as chromosphere bases of magnetic field lines that form an external shell (braid) of the CME at the late stage of the flare.     

Neutral surfaces of coronal magnetic field and solar filaments

The shape of solar filaments is compared with the projection of parts of the neutral surface of the coronal magnetic field within a certain range of heights at different aspects of observation due to the rotation of the Sun. Neutral surfaces are calculated in the potential approximation from the photospheric data. The comparison shows that the material of filaments is concentrated mainly near the neutral surface of the potential field. The traces of the neutral surface section by the horizontal plane serve as polarity inversion lines (PILs) of the vertical field at the given height. In projection onto the disk, a lower edge of the filament with the intermediate barbs protruding on each side is delineated by the PIL at the low height, while an upper edge touches the high-height PIL. All material of the filament is enclosed in the space between these two lines. Although in reality the magnetic field structure near filaments differs very strongly from the potential field structure, their neutral surfaces can be similar and close, especially at low heights. This fact is probably the cause of the observed correlation. It can be used to determine the height of the upper edge of filaments above the photosphere in the case of observations only on the disk.     

最小间隔安全性的定量评估

在空中交通服务（简称为“ATS”,下同）中,最小间隔的安全性评估是防相撞工作的重要一环,直接关系到空域安全余度与容量效能的平衡关系。我国长期以来采用经验型定性评估为主,缺少定量评估支撑;最小间隔的科学性、合理性大打折扣。通过文献研读,本文根据Reich碰撞危险模型（简称为“Reich模型”,下同）,对最小间隔的安全性进行了定量评估,以期改善此方面工作。     

Vertical structure of the magnetic field in active regions of the sun at coronal heights

High-altitude measurements and magnetic field distribution in active regions are always an important problem to verify existing models at heights from units to hundreds of Mm. Optical methods of analysis of the magnetic structure work well only at the photosphere level. At the same time, the progress of radio astronomy methods of analyzing the solar radio emission [1] and of the theory of solar plasma radiation [2] facilitates introduction of new methods for measuring the magnetic field strength at various altitudes in the solar atmosphere. In this paper we use multi-wave observations of polarization of the radio emission of active regions in the microwave range together with precise magnetosphere data in order to develop a method of projection for measuring the height distribution of the magnetic field.     

Features of RadioAstron Mission Control

Support means of the Spektr-R spacecraft flight and features of the Mission Control Center operation and spacecraft control are considered. Software for scheduling and preparing sessions of controlling and simulating for the spacecraft operation are considered. The problems of ballistic navigation support of the spacecraft flight are presented. Ground spacecraft control segment and software for analyzing and imaging telemetric information are considered.     

Identification of coronal sources of the solar wind from solar images in the EUV spectral range

Methods of localizing coronal sources of the solar wind (SW), such as coronal holes, quasi-stationary fluxes from active regions, and transient sources associated with small-scale active phenomena are considered based on vacuum-ultraviolet (EUV) images of the corona at low solar activity during the initial period of the 24th solar cycle (2010). It is shown that a SW velocity profile can be calculated from the relative areas of coronal holes (CH) at the central part of the disk based on the images in the ranges of 193 and 171 Å. The images in the 193 Å describe the geometry of large HCs that represent sources of fast SW well. The images in 171 Å are a better visualization of small CHs, based on which the profile of a slow SW component was calculated to a high accuracy (up to 65 km/s). According to Hinode/EIS data of October 15, 2010, using the Doppler spectroscopy method at the streamer base over the active region 11112, the source of the outgoing plasma flux with the mean velocity of 17 km/s was localized in the magnetic field region with an intensity of less than 200 Gauss. According to the estimate, the density of the plasma flux from this source is an order of magnitude greater than the value required for explaining the distinction between the calculated and measured profiles of a slow SW velocity. For finding the transient SW component based on small-scale flare activity, SW parameters were analyzed for the periods of flares accompanied by coronal mass ejections (CMEs), and for the periods without flares, according to the data obtained in 2010 from the ACE and GOES satellites and by coronagraphs on the STEREO-A and -B spacecraft. The ion ratios C⁺⁶/C⁺⁵ and O⁺⁷/O⁺⁶ and the mean charge of Fe ions for periods with flares were shown to be shifted toward large values, suggesting the presence of a hot SW component associated with flare activity. A noticeable correlation between the maximum charge of Fe ions and the peak power of a flare, previously observed for flares of a higher class, was confirmed. The mean value of the SW flux density during the periods of flares was 30% higher than that in the periods without flares, which is possibly associated also with the growth of fluxes from other sources with an increasing solar activity level. Based on the example of a series of flares of October 13–14, 2010, it was supposed that transient SW fluxes from the weak flares at low solar activity can manifest themselves in the form of interplanetary ICME-transients.     

钝感GAP微烟推进剂的能量性能计算

根据推进剂配方理论计算程序计算了含N-脒基脲二硝酰胺(FOX-12)、1,1-二氨基-2,2-二硝基乙烯(FOX、7)、3-硝基-1,2,4-三唑-5-酮(NTO)、三氨基三硝基苯(TATB)、3,4-二硝基呋咱基氧化呋咱(DNTF)、黑索今(RDX)、二硝酰胺铵(ADN)等高能钝感氧化剂及1,2,4-丁三醇三硝酸酯(BTTN)、二缩三乙二醇二硝酸酯(TEGDN)、三羟甲基乙烷三硝酸酯(TMETN)、N-丁基-2-硝酸酯乙基硝胺(Bu-NENA)等钝感增塑剂的几种单元推进剂和钝感微烟推进剂的能量性能.计算结果表明,所列的7种含能氧化剂中,由RDX和DNTF形成的单元推进剂的标准理论比冲分别为2 696.4 N·s/kg和2 610.2 N·s/kg,明显优于其他几种氧化剂.当采用DNTF部分取代GAP推进剂中的RDX或ADN后,推进剂的理论比冲、密度和特征速度相应提高.由于DNTF的感度低于RDX,因此DNTF引入推进剂中,对提高钝感GAP微烟推进剂的能量性能是有益的.     

Preliminary results of Texus 8 experiments on effects of surface tension minimum

A stable, observable liquid-gas interface was realized in an experimental cell (3 × 2 × 1 cm) under microgravity conditions. The liquid used was an aqueous 6.24 10^?3 molal solution of n-heptanol. A temperature gradient, established at the interface, resulted in the build-up of a Marangoni convection cell with the liquid flowing in an unusual direction (i.e. at the surface the liquid flowed from the cold to the hot side).The same experiment on Earth gives rise to a Marangoni cell superimposed on buoyancy cells. The Marangoni and the buoyancy cells then turn in opposite directions.     

嫦娥二号卫星的四大特点

<正>在嫦娥一号卫星发射后不到3年的时间里,嫦娥二号卫星就顺利升空。虽然其主要设备继承了嫦娥一号卫星,但它在我国卫星型号快速研制方面积累了     

当代创新的五个社会特征

本文以当代世界科技创新活动为背景，分析了当代创新的社会性、效用性、时效性、持续性和系统性。     

SPOT-5卫星系统性能概述

概要介绍SPOT - 5卫星的主要成像传感器 ,精确定位技术及数据格式。介绍分析卫星数据的应用前景     

Selection of Salient Features for Route Directions

People navigating in unfamiliar environments rely on wayfinding directions, either given by people familiar with the place, or given by maps or wayfinding services. The essential role of landmarks in human route communication is well-known. However, mapping the human ability to select landmarks ad hoc for route directions to a computational model was never tried before. Wayfinding services manage the problem by using predefined points of interest. These points are not automatically identified, and they are not related to any route. In contrast, here a computational model is presented that selects salient features along a route where needed, e.g., at decision points. We propose measures to formally specify the salience of a feature. The observed values of these measures are subject to stochastical tests in order to identify the most salient features from datasets. The proposed model is implemented and checked for computability with a use case from the city of Vienna. It is also crosschecked with a human subject survey for landmarks along a given route. The survey provides evidence that the proposed model selects features that are strongly correlated to human concepts of landmarks. Hence, integrating the selected salient features in wayfinding directions will produce directions with lower cognitive workload and higher success rates, compared to directions based only on geometry, or on geometry and static points of interest.     

粒度和形貌及粒度分布对RDX安全和热分解性能的影响

采用溶剂/非溶剂法和筛分法,通过控制搅拌速度及溶剂与非溶剂温度差,制备了不同粒度、形貌和粒度分布的RDX粉末。利用激光粒度仪、扫描电子显微镜(SEM)和X射线衍射(XRD)对其进行了相应表征;利用撞击和摩擦感度试验、慢烤试验及DSC测试分别研究了不同粒度、形貌及粒度分布的RDX样品的安全性能和热分解特性。研究结果表明,粒度、形貌及粒度分布是影响RDX安全和热分解性能的重要因素。随着粒度的减小,RDX的机械和热感度显著降低。另外,窄粒度分布的RDX样品普遍具有更低的机械感度,而宽粒度分布的RDX样品通常具有更好的热稳定性。     

高原机场雷达管制工作中的几项特点

昆明机场自实施雷达管制一年多来，能更好地适应空中流量的增长，满足了昆明日益增长的流量要求。通过成立进近管制室，划分进近扇区，有效地分离了以前繁杂的工作程序，降低了管制员的工作负担，也使安全得到了更好的保障。     

Influence of a surface tension minimum as a function of temperature on the marangoni convection

Aqueous long chain alcohol solutions have a surface tension which presents a minimum as a function of the temperature. At this particular temperature, the dimensionless Marangoni number is vanishing. It is thus expected that around the temperature of the minimum, Marangoni Convection would be slowered with a convective pattern deeply modified. An experiment to be performed in microgravity during the Texus 8 flight is described.     

前苏联/俄罗斯火星探测器研制特点

介绍了前苏联/俄罗斯火星探测器概况,分析了其火星探测器太阳电池阵、结构、测控、推进、热控,以及综合测试等分系统的先进技术特点与设计理念.其产品的模块化、测试的自动化、优化的发射流程可为我国未来火星探测项目提供借鉴.     

Some Features of Vibrational Perturbations onboard the MirOrbital Station

A number of scientific and technical experiments were carried out and are still being carried out onboard the Mirorbital station in various fields: physics of fluids, space materials study, astrophysics, biotechnology, and so on. The quality and reliability of space experiments are essentially dependent on a knowledge of real microgravitational situation onboard a satellite, which essentially depends on vibrational perturbations. A lot of vibration processes studies have been done up to now on the Mirstation in the following lines of research: control of dynamic and exploitation regimes when carrying out biotechnological and technological experiments; determination of the contribution of different onboard systems and mechanisms to the total vibration perturbations power; and investigation of distributions of microacceleration levels and dynamics of vibration processes in different modules and segments of the orbital station. This paper presents the results of the analysis of vibration perturbations produced by some standard onboard Mirstation systems in a configuration when the KVANT-2 and KRISTALL modules were arranged along the yaw axis of the mainframe. It is shown that due to strong requirements for tolerable levels of the microaccelerations onboard the International Space Station (ISS), the investigations of microgravitational situation, as an integral part of the technological environment, now have a high priority.     

工艺标准化在批生产中的作用

概述了先进的工业化国家武器系统及航天产品批生产组织与工艺标准化工作的关系,阐述了批量生产以成组技术为基础开展工作的观点及工艺标准化工作在批量生产质量控制中的重要作用,对航天企业在批量生产前后需开展和完善的工艺标准化工作的一些内容及对工艺标准化机构和人员素质的要求提出了建议。